Stefan-Boltzmann law (Stefan, L. Boltzmann)
By Nick Greene, About.com
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STEFAN-BOLTZMANN LAW - Law of blackbody radiation that states that the amount of energy given off by a blackbody per second per unit area (flux) is proportional to the fourth power of the temperature of the blackbody.
Stefan-Boltzmann law (Stefan, L. Boltzmann)
The radiated power P (rate of emission of electromagnetic energy) of a hot body is proportional to the radiating surface area, A, and the fourth power of the thermodynamic temperature, T.
Stefan-Boltzmann Law - The relationship between the temperature of a blackbody and the rate at which it emits radiant energy ...
[edit] Stefan-Boltzmann law
Main article: Stefan-Boltzmann law
This law states that amount of thermal radiations emitted per second per unit area of the surface of a black body is directly proportional to the fourth power of its absolute ...
Stefan-Boltzmann Law - This law is used for black bodies, perfect radiation (light) emitters and absorbers and indicates how much total energy they give off.
Stefan-Boltzmann Law
You make a light in the world and you hope someone can still look up from the dust for long enough to see it
Planck's constant ...
Stefan-Boltzmann Law - (n.)
The radiation law that states that the energy emitted by a black body varies with the fourth power of the temperature.
Stellar epoch - (n.) ...
The Stefan-Boltzmann law potentially gives us a way of determining the radius of star. We can determine the temperature by means of the peak in the blackbody spectrum. Next we can measure the amount of energy received here at the Earth.
3. Stefan-Boltzmann Law, which relates the total energy emitted (E) to the absolute temperature (T).
In the image above, notice that: ...
Stefan-Boltzmann law relation between the amount of energy emitted by a unit area on an object producing a thermal spectrum and its temperature: energy in Joules emitted by one square meter = 5.67× 10-8 × temperature4.
between emission and absorption of any given wavelength at a given temperature; (b) the Planck law describes the variation of intensity of black-body radiation at a given temperature, as a function of wavelength; (c) the Stefan-Boltzmann law relates ...
In astrophysics, a measure of the temperature of a star deduced by means of the Stefan-Boltzmann law, from the total energy emitted per unit area. Compare brightness temperature, color temperature.
1879: Stefan-Boltzmann law formulated empirically omega_T^4
1880s & 1890s: Lord Rayleigh and Wilhelm Wien both solve part of the blackbody equation, but both solutions are approximations that "blow up" out of their useful ranges.
He used it to estimate the effective temperature of the Sun at 6,000 K which was much closer than the previous estimate of 10,000 K predicted using the Stefan-Boltzmann law of radiation.
The total luminosity of the sun is given by the Stefan-Boltzmann Law (above), which for the sun works out to 3.85x1026 J/s (approximately what is given on the opening page of this section, which is a value taken from NASA).
 See also: Solar, Temperature, Energy, Field, Astronomy
  
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